太阳活动区的观测与分析

发布时间：2018-01-11 18:32

本文关键词：太阳活动区的观测与分析　出处：《中国科学院研究生院(云南天文台)》2016年硕士论文　论文类型：学位论文

【摘要】：太阳作为离我们最近的一颗恒星,不但为我们带来了光明和温暖,也影响着我们生活的方方面面。对太阳的研究一直是天文学的一个重要分支。太阳活动区通常指太阳上强磁场周围活动现象比较频繁的区域。随着观测手段以及技术水平的提高,尤其是越来越多的高分辨率空间和地面太阳望远镜投入使用,使我们采集到了大量的太阳活动区数据,也发现了许多令人惊奇的太阳活动现象。这些太阳活动现象不仅与空间天气以及地球气候状况有着非常密切的联系,而且也为我们研究基础空间极端条件下等离子体表现提供了大量的数据基础。太阳活动区内存在着黑子、耀斑、日珥和日冕物质抛射等多种现象,这些现象的存在都与太阳磁场有密切的联系。首先磁场可以提供的磁压力和磁张力来支撑太阳大气中致密的等离子体物质,从而使其可以保持在空中不会因为重力而下落;其次磁场也可以在一定程度上阻碍热交换,这就使得冷的等离子体也可以稳定的存在于更热的太阳大气之中;最后磁场中储存的磁能如果被释放出来则可以驱动剧烈的太阳活动现象。但是由于太阳活动区复杂的大气环境和磁场中等离子体本身复杂的特性,太阳活动区内详细的物理过程和演化规律一直没有被很好的理解。更加详细的研究以及更加深入的分析,毫无疑问都需要更多的观测数据和观测现象作为基础。围绕大量的太阳活动区高时间和空间分辨率的观测数据,我们对太阳活动区内的一些典型的现象进行了一些分析和研究。这里我们呈现了几个不同种类爆发暗条周围磁场衰减指数的空间分布情况。对比的结果表明不同种类的爆发暗条周围磁场衰减指数的分布也有着一定的区别。我们还首次发现部分爆发暗条周围存在衰减指数分布反常的区域,在这些反常的区域呈现出上下相邻的两个斑块,它们具有着相对陡峭的衰减指数,观测也表明这些异常的区域同暗条发生爆发断裂的位置有着良好的对应关系。对磁场拓扑结构的分析则表明这些衰减指数分布反常的区域中磁场联通性有着很强烈的变化,更进一步分析表明这些磁场衰减指数分布异常的区域位于某些特殊的准磁分界层(QSL),而在准分界层和衰减指数异常区域的分布的关系以及物理模型方面我们也做了一定的研究,也提出了一种可能的模型来解释这类典型的部分暗条爆发现象。此外我们也研究了2015年6月18日发生的一个很明显的冕环振荡事件。观测结果表明相邻的一束冕环中不同冕环的振荡情况有着很大的不同,它们的周期和振幅都存在着很大的差异。另外我们也发现同一个冕环不同位置的振荡也有着明显的差别,在远离耀斑源的位置的振荡经历了一个阻尼过程,而靠近耀斑源的那部分冕环振动幅度则有着一个增加的过程,我们对此进行了简单的理论分析,结果表明该现象可能是由于冕环不同位置受到冲击的角度的不同所产生。最后我们还针对相位一致性方法增强图像提出一个新的冕环识别方法(简称PCB),该方法依据冕环形态变化比较平缓的形态学特性,将冕环识别方向限制在一个较小的范围之内,并且首次将识别过程中推进方向的变化情况和识别点的相位一致性大小同时作为终止识别的判据。对多组数据的识别和分析则表明相位一致性方法增强的图像的确很适合被用于冕环识别,而我们提出的PCB方法所识别的冕环结构则同时有着很好的完整性和准确性,是一套现实可行的冕环自动识别方法。
[Abstract]:The sun as a star from us recently, not only bring us a bright and warm, also affects every aspect of our lives. The study on the sun has been an important branch of astronomy. The solar active region on the sun usually refers to a strong magnetic field around the activities more frequent area. With the means of observation and to improve the technical level, especially more and more high resolution space and ground-based solar telescope is put into use, we collected a large amount of data on solar activity, also discovered many amazing solar activities. These solar activities not only has a close relationship with the space weather and climate conditions, but also provides a data foundation for us to study basic space plasmas under extreme conditions. Solar activity in the region there are sunspots, flares, and coronal prominence Mass ejections and other phenomena, these phenomena are connected with the solar magnetic field. The first magnetic pressure and magnetic tension can be provided to support the dense plasma substance in the solar atmosphere, so that it can keep in the air will not fall because of gravity; the magnetic field can also impede heat exchange in a certain extent, which makes the cold plasma can also exist in the hot atmosphere of the sun; finally the magnetic field in the stored magnetic energy is released if can be driven by intense solar activity phenomena. But because of the characteristics of the atmospheric environment of solar active region and complex magnetic field plasma complex, solar activity in the region with the physical the process of evolution and has not been well understood. More detailed study and more in-depth analysis, there is no doubt that it needs more data And observations as a basis. The observation data around the high spatial and temporal resolution of the solar active region on the sun, our activities in the area of some typical phenomena are analyzed and studied. Here we present several different types of filament eruption around the distribution of magnetic field attenuation index space. The results indicate that the different types of the outbreak of a dark ambient magnetic field attenuation index distribution also have some differences. We also found that for the first time around a part of the outbreak of the dark decay index distribution of anomalous region in these anomalous area exhibits two patches on adjacent, they have a relatively steep attenuation index, the observation also shows that these abnormal with the occurrence of fracture occurred in the dark region position has a good corresponding relation. The analysis of magnetic field topology indicates that these anomalous attenuation index distribution In the area of the magnetic field has a very strong Unicom changes, further analysis shows that the magnetic field attenuation index abnormal distribution area is located in some special quasi magnetic boundary layer (QSL), and in the relationship between quasi boundary layer and attenuation distribution index abnormal area and the physical model we also do some research, also put forward a possible model to explain this kind of typical part of the filament explosion phenomenon. In addition, we also study a very obvious coronal loop oscillations of incidents in June 18, 2015. The observation results showed that the different coronal loop oscillations of a coronal loop in adjacent beam is very different, their period and amplitude there is a big difference. We also found the same coronal loop oscillations in different positions have obvious difference, a damping process in the oscillation source location away from the flare, but close to Yao The crown ring spot source vibration amplitude has an increase in the process, we conducted a simple theoretical analysis results show that this phenomenon may be due to the impact of the coronal loop in different positions of different angles generated. Finally we also according to the method of phase congruency enhanced image and proposed a new crown loop identification method (PCB), the method based on morphological characteristics of coronal loop morphological changes slowly, the coronal loop recognition within the limits of a smaller range, and for the first time, the consistency of phase size in the process of recognition of the advancing direction changes and recognition at the same time as the termination criterion. The identification and analysis of recognition the multi group data show that the image enhancement method of phase congruency is very suitable to be used in coronal loop recognition, coronal loop structure of PCB we put forward the method of recognition is also a good end Integrity and accuracy are a practical and feasible method for automatic identification of coronal rings.

【学位授予单位】：中国科学院研究生院(云南天文台)
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P182

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